Results 21 to 30 of about 553,339 (197)

Searching for signatures of planet formation in stars with circumstellar debris discs [PDF]

, 2015
(Abridged) Tentative correlations between the presence of dusty debris discs and low-mass planets have been presented. In parallel, detailed chemical abundance studies have reported different trends between samples of planet and non-planet hosts.
Eiroa, C., Maldonado, J., Montesinos, B., Mora, A., Villaver, E.   +4 more
core   +4 more sources

A Chandra X-ray study of the young star cluster NGC 6231: low-mass population and initial mass function [PDF]

, 2016
NGC6231 is a massive young star cluster, near the center of the Sco OB1 association. While its OB members are well studied, its low-mass population has received little attention.
Damiani, F., Micela, G., Sciortino, S.
core   +2 more sources

On Low Mass AGB Stars [PDF]

Symposium - International Astronomical Union, 1991
Recent results on low mass AGB stars are presented. Observed amounts of AGB mass loss imply that thermal pulses will only be encountered for stars of initial mass less than about 4M⊙ for Pop I and 3 M⊙ for Pop II. Mc – L, Me – τif, and Mc – Tb relations are summarized.
I.-Juliana Sackmann, Arnold I. Boothroyd
openaire   +1 more source

High-redshift galaxies and low-mass stars [PDF]

, 2014
The sensitivity available to near-infrared surveys has recently allowed us to probe the galaxy population at z ≈ 7 and beyond. The existing Hubble Wide Field Camera 3 (WFC3) and Visible and Infrared Survey Telescope for Astronomy (VISTA) Infrared Camera (
Bremer, Malcolm N, Stanway, Elizabeth R, Wilkins, Stephen M   +2 more
core   +2 more sources

Efficiencies of Low‐Mass Star and Star Cluster Formation

The Astrophysical Journal, 2000
20 pages, 2 figures, accepted by ...
Matzner, Christopher D., McKee, Christopher F.   +1 more
openaire   +2 more sources

Low-mass companions to Hyades stars

, 2005
It is now well established that a large fraction of the low-mass stars are binaries or higher order multiples. Similarly a sizable fraction have giant planets.
A. P. Hatzes, Abt, B. Macintosh, Boesgaard, Burrows, Cayrel, Chabrier, Chauvin, Chauvin, Close, Cochran, D. B. Paulson, Dahn, Duquennoy, E. W. Guenther, Endl, Fischer, Freed, Ghez, Goto, Guenther, Guenther, Henry, J. Patience, Kirkpatrick, Lebreton, Lineweaver, Liu, Lowrance, Lowrance, Malkov, Martín, Martín, Masciadri, Masciadri, Mazeh, Mazeh, McCarthy, McCaughrean, Nakajima, Neuhäuser, Neuhäuser, Neuhäuser, Neuhäuser, Patience, Paulson, Paulson, Paulson, Perryman, Potter, Reid, Santos, Seifahrt, Stern, Tinney, Torres, Udry, W. D. Cochran, Wuchterl, Zapatero Osorio, Zucker   +60 more
core   +1 more source

The Rotational Evolution of Young, Binary M Dwarfs [PDF]

, 2018
We have analysed K2 light curves for more than 3,000 low mass stars in the $\sim$8 Myr old Upper Sco association, the $\sim$125 Myr age Pleiades open cluster and the $\sim$700 Myr old Hyades and Praesepe open clusters to determine stellar rotation rates.
Barrado, David, Bouvier, Jerome, Cody, Ann Marie, David, Trevor, Hillenbrand, Lynne, Pinsonneault, Marc, Rebull, Luisa, Stauffer, John   +7 more
core   +5 more sources

X-ray observations of eight young open star clusters : I. Membership and X-ray Luminosity

, 2013
We present a detailed investigation of X-ray source contents of eight young open clusters with ages between 4 to 46 Myr using archival X-ray data from XMM-Newton. The probable cluster memberships of the X-ray sources have been established on the basis of
Bhatt, Himali, Kumar, Brijesh, Pandey, J. C., Sagar, Ram, Singh, K. P.   +4 more
core   +1 more source

Low Mass Stars or Intermediate Mass Stars? The Stellar Origin of Presolar Oxide Grains Revealed by Their Isotopic Composition

Frontiers in Astronomy and Space Sciences, 2021
Among presolar grains, oxide ones are made of oxygen, aluminum, and a small fraction of magnesium, produced by the 26Al decay. The largest part of presolar oxide grains belong to the so-called group 1 and 2, which have been suggested to form in Red Giant
S. Palmerini, S. Palmerini, S. Cristallo, S. Cristallo, M. Busso, M. Busso, M. La Cognata, M. L. Sergi, M. L. Sergi, D. Vescovi, D. Vescovi, D. Vescovi   +11 more
doaj   +1 more source

Chemical abundances of stars with brown-dwarf companions

, 2014
It is well-known that stars with giant planets are on average more metal-rich than stars without giant planets, whereas stars with detected low-mass planets do not need to be metal-rich.
Hernández, J. I. González, Israelian, G., Sahlmann, J., Santos, N. C., Sánchez, D. Mata, Udry, S.   +5 more
core   +1 more source